The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters
We examine the kinematic morphology of early-type galaxies (ETGs) in eight galaxy clusters in the Sydney-AAO Multi-object Integral-field spectrograph Galaxy Survey. The clusters cover a mass range of $14.2\,\lt \mathrm{log}({M}_{200}/{M}_{\odot })\lt 15.2$ and we measure spatially resolved stellar k...
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ftanucanberra:oai:openresearch-repository.anu.edu.au:1885/218517 2024-01-14T10:10:28+01:00 The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters Brough, Sarah van de Sande, J Owers, Matthew D'Eugenio, Francesco Sharp, Rob Cortese, L Scott, Nicholas Medling, Anne Sweet, Sarah Bland-Hawthorn, Joss Bryant, J. Drinkwater, Michael John Tonini, C Lawrence, J Lawrence, J S Richards, Samuel application/pdf http://hdl.handle.net/1885/218517 https://doi.org/10.3847/1538-4357/aa7a11 en_AU eng IOP Publishing 0004-637X http://hdl.handle.net/1885/218517 doi:10.3847/1538-4357/aa7a11 The Astrophysical Journal Journal article ftanucanberra https://doi.org/10.3847/1538-4357/aa7a11 2023-12-15T09:36:14Z We examine the kinematic morphology of early-type galaxies (ETGs) in eight galaxy clusters in the Sydney-AAO Multi-object Integral-field spectrograph Galaxy Survey. The clusters cover a mass range of $14.2\,\lt \mathrm{log}({M}_{200}/{M}_{\odot })\lt 15.2$ and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses $10.0\lt \mathrm{log}({M}_{* }/{M}_{\odot })\leqslant 11.7$ within 1 R 200 of the cluster centers. We calculate the spin parameter, λ R , and use this to classify the kinematic morphology of the galaxies as fast or slow rotators (SRs). The total fraction of SRs in the ETG population is F SR = 0.14 ± 0.02 and does not depend on host cluster mass. Across the eight clusters, the fraction of SRs increases with increasing local overdensity. We also find that the slow-rotator fraction increases at small clustercentric radii (R cl < 0.3 R 200), and note that there is also an increase in the slow-rotator fraction at R cl ~ 0.6 R 200. The SRs at these larger radii reside in the cluster substructure. We find that the strongest increase in the slow-rotator fraction occurs with increasing stellar mass. After accounting for the strong correlation with stellar mass, we find no significant relationship between spin parameter and local overdensity in the cluster environment. We conclude that the primary driver for the kinematic morphology–density relationship in galaxy clusters is the changing distribution of galaxy stellar mass with the local environment. The presence of SRs in the substructure suggests that the cluster kinematic morphology–density relationship is a result of mass segregation of slow-rotating galaxies forming in groups that later merge with clusters and sink to the cluster center via dynamical friction. Article in Journal/Newspaper sami Australian National University: ANU Digital Collections The Astrophysical Journal 844 1 59 |
institution |
Open Polar |
collection |
Australian National University: ANU Digital Collections |
op_collection_id |
ftanucanberra |
language |
English |
description |
We examine the kinematic morphology of early-type galaxies (ETGs) in eight galaxy clusters in the Sydney-AAO Multi-object Integral-field spectrograph Galaxy Survey. The clusters cover a mass range of $14.2\,\lt \mathrm{log}({M}_{200}/{M}_{\odot })\lt 15.2$ and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses $10.0\lt \mathrm{log}({M}_{* }/{M}_{\odot })\leqslant 11.7$ within 1 R 200 of the cluster centers. We calculate the spin parameter, λ R , and use this to classify the kinematic morphology of the galaxies as fast or slow rotators (SRs). The total fraction of SRs in the ETG population is F SR = 0.14 ± 0.02 and does not depend on host cluster mass. Across the eight clusters, the fraction of SRs increases with increasing local overdensity. We also find that the slow-rotator fraction increases at small clustercentric radii (R cl < 0.3 R 200), and note that there is also an increase in the slow-rotator fraction at R cl ~ 0.6 R 200. The SRs at these larger radii reside in the cluster substructure. We find that the strongest increase in the slow-rotator fraction occurs with increasing stellar mass. After accounting for the strong correlation with stellar mass, we find no significant relationship between spin parameter and local overdensity in the cluster environment. We conclude that the primary driver for the kinematic morphology–density relationship in galaxy clusters is the changing distribution of galaxy stellar mass with the local environment. The presence of SRs in the substructure suggests that the cluster kinematic morphology–density relationship is a result of mass segregation of slow-rotating galaxies forming in groups that later merge with clusters and sink to the cluster center via dynamical friction. |
format |
Article in Journal/Newspaper |
author |
Brough, Sarah van de Sande, J Owers, Matthew D'Eugenio, Francesco Sharp, Rob Cortese, L Scott, Nicholas Medling, Anne Sweet, Sarah Bland-Hawthorn, Joss Bryant, J. Drinkwater, Michael John Tonini, C Lawrence, J Lawrence, J S Richards, Samuel |
spellingShingle |
Brough, Sarah van de Sande, J Owers, Matthew D'Eugenio, Francesco Sharp, Rob Cortese, L Scott, Nicholas Medling, Anne Sweet, Sarah Bland-Hawthorn, Joss Bryant, J. Drinkwater, Michael John Tonini, C Lawrence, J Lawrence, J S Richards, Samuel The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters |
author_facet |
Brough, Sarah van de Sande, J Owers, Matthew D'Eugenio, Francesco Sharp, Rob Cortese, L Scott, Nicholas Medling, Anne Sweet, Sarah Bland-Hawthorn, Joss Bryant, J. Drinkwater, Michael John Tonini, C Lawrence, J Lawrence, J S Richards, Samuel |
author_sort |
Brough, Sarah |
title |
The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters |
title_short |
The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters |
title_full |
The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters |
title_fullStr |
The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters |
title_full_unstemmed |
The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters |
title_sort |
sami galaxy survey: mass as the driver of the kinematic morphology-density relation in clusters |
publisher |
IOP Publishing |
url |
http://hdl.handle.net/1885/218517 https://doi.org/10.3847/1538-4357/aa7a11 |
genre |
sami |
genre_facet |
sami |
op_source |
The Astrophysical Journal |
op_relation |
0004-637X http://hdl.handle.net/1885/218517 doi:10.3847/1538-4357/aa7a11 |
op_doi |
https://doi.org/10.3847/1538-4357/aa7a11 |
container_title |
The Astrophysical Journal |
container_volume |
844 |
container_issue |
1 |
container_start_page |
59 |
_version_ |
1788065178778075136 |